Discussion on access to observatories

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TRANSNATIONAL ACCESS ACTIVITIES
Discussion on access to observatories Purpose I
mplementation of a Virtual Observatory with a
collection of Cosmic Rays and High-Energy Gamma
Rays data archives and software tools to form a
scientific research environment in which
multi-messenger astroparticle research programs
can be conducted. A.Morselli, INFN
University of Roma Tor Vergata
HEAPnet meeting Amsterdam, 19-20 February, 2007
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Energy versus time for X and Gamma ray detectors
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Sensitivity of g-ray detectors
High galactic latitudes (background Fb2 10-5 g
cm-2 s-1 sr -1 (100 MeV/E)1.1). Cerenkov
telescopes sensitivities (Veritas, MAGIC,
Whipple, Hess, Celeste, Stacee, Hegra) are for 50
hours of observations. Large field of view
detectors sensitivities (AGILE, GLAST, Milagro,
ARGO) are for 1 year of observation.
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TA1 Access to Virtual Data(TA-ViDa1 )
MUNICH
PARIS
H.E.S.S.
MAGIC
ROMA
AGILE PAMELA GLAST
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TA1 Access to Virtual Data (TA-ViDa1 )
Location (town, country) Roma
Web site address www.roma2.infn.it
Legal name of organisation operating the infrastructure INFN
Location of organisation (town, country) Roma , Italy
Approximate investment/ replacement cost of the infrastructure to which access is offered () gt 72,5 M
Annual operating costs (excl. investment costs) of the infrastructure () 1.5 M
Funding sources that cover those operating costs INFN, ASI, MIUR
Contract number under FP5 and/or FP6, if any
Coordinator Aldo Morselli
Requested Budget 549 020
The Roma Computing Center in Rome Tor Vergata
will have the task to support the storage, the
management and the utilization of the PAMELA Data
Archive and AGILE and GLAST Data Archive Mirrors
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TA1 Access to Virtual Data (TA-ViDa1
)(cont.)
Location (town, country) Munich
Web site address www.mppmu.mpg.de
Legal name of organisation operating the infrastructure MPI-M
Location of organisation (town, country) Munich, Germany
Approximate investment/ replacement cost of the infrastructure to which access is offered () 8,0 M
Annual operating costs (excl. investment costs) of the infrastructure () 0.8 M
Funding sources that cover those operating costs MPG (Max-Planck-Society)
Contract number under FP5 and/or FP6, if any
Coordinator Masahiro Teshima i
Requested Budget 70 370
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TA1 Access to Virtual Data (TA-ViDa1
)(cont.)
Location (town, country) Paris
Web site address www.mppmu.mpg.de
Legal name of organisation operating the infrastructure cc.in2p3.fr
Location of organisation (town, country) IN2P3/CNRS
Approximate investment/ replacement cost of the infrastructure to which access is offered () 10,0 M
Annual operating costs (excl. investment costs) of the infrastructure () 0.9 M
Funding sources that cover those operating costs IN2P3/CNRS
Contract number under FP5 and/or FP6, if any
Coordinator Arache Djannati-Atai
Requested Budget 70 370
Total 689 760
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Transnational Access

• Access to and exchange of data
• A ( web-based) database of astro-particle
  observations and the exchange of
  inter-disciplinary data
• Computer modelling and simulations

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expected impact

• Correlate observations of space experiments
  (AGILE, GLAST) and ground observations
• ( H.E.S.S., MAGIC, ARGO).
• Multi-wavelengths programs including x-rays,
  radio, IR, Optical ....
• Develop observation methods for transient
  sources alert systems and combination of space
  and ground observations .
• Correlate ? observations with ? and CR
  observations.
• Evaluate potential discovery and physics outcome.

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• Description of work
• Multiwavelength (MW) studies are intimately
  related to essentially all the astrophysical
  topics of gamma-ray astrophysics. All of the
  gamma ray observations will require observational
  programs at other wavelengths to extract their
  full value.
• We envision three types of multiwavelength
  study
• identification of sources in known classes, such
  as blazars and pulsars,
• ii) discovery of new sources classes,
• iii) intensive, MW explorations of the brightest
  and most variable sources that will allow deep
  study of the source physics.

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Milestones

• after 18 months
• Definition of a Coordination between ground and
  space gamma ray observatories
• ii) Definition of a Coordination between existing
  MW programs such as
• Whole Earth Blazar Telescope WEBT
• (http//www.to.astro.it/blazars/webt/homepage.html
  ).
• and/or
• European Network for the Investigation of
  Galactic Nuclei through Multifrequency Analysis
  ENIGMA (http//www.lsw.uni heidelberg.de/users/s
  wagner/enigma.html).
• and space and ground gamma-ray observation

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Advantages of a Virtual Observatory

• The advantages of a Virtual Observatory approach
  are several.
• The data collected by each high energy experiment
  can be used multiple times by different teams and
  for different scientific purposes, thus
  increasing the overall efficiency.
• The data are collected in a controlled and
  uniform fashion, ensuring long-term scientific
  utilization by different users.
• The worldwide accessibility via web to the
  Virtual Observatory makes it a powerful
  scientific source that is available to any
  community, including those that are economically
  disfavoured.
• A Virtual Observatory can also be used
  as a powerful and stimulating educational tool.

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• once the Virtual Observatory is in operation,
  other experiments and other centers could be
  interested to join it.

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Roma Computing Center

• The Roma Computing Center is located in the
  Department of Physics at the University of Rome
  Tor Vergata.
• The infrastructure construction started in summer
  2004 and is in its final setup phase thanks to
  INFN, ASI and MIUR funding. It will be fully
  operative by the end of 2005, in order to be
  ready for reception, distribution, analysis and
  storage of data of the PAMELA instrument. The
  expected PAMELA data flow is approximately 8
  Gbyte/day.
• In Feb.2006 AGILE satellite should be in orbit
  and starting to send data to the Center. The
  expected AGILE data flow is approximately
  6Gbyte/day.
• The Center is near the INFN Clean-Rooms facility,
  where the Pamela Flight Model has been
  integrated. Its location in the contest of the
  University of Rome Tor Vergata
  (www.fisica.uniroma2.it) ensures a very
  stimulating scientific environment, from which
  visiting scientists may benefit.
• An user room with different working stations
  which permits a collaborative work is already
  operative. The main hardware components of the
  Roma Computing Center are a 20 TByte storage
  system a back-up system 10 double 3.2 GHz
  processor computers.
• The Center is connected to the main INFN computer
  center (CNAF, http//www.cnaf.infn.it/) for any
  need of storage and CPU computer power .
• CNAF is integrated in the European Data-Grid
  network

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Paris Data Center

• The Paris Data Center is located at the APC
  (Astroparticle and Cosmology) Laboratory and is
  dedicated to multi-wavelength studies in a wide
  energy range starting from radio to very high
  energy gamma-rays. The current setup includes a
  double 3.2 GHz processor computer with TByte
  storage capacity at APC as an interface to the
  Center for Computing of In2p3 (CCPN/Lyon,
  http//cc.in2p3.fr/) through a fast connection.
  The H.E.S.S. Data processing and storage consumes
  about 7 of CCPN/Lyon total capacity which has
  about 1 TFlops of computing power (200 3 GHz
  PCs) and 20280 TB (disks tapes).

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Munich Data Center

• The Munich Data Center is located at the Max
  Planck Institute for Physics and it is mainly
  dedicated to the MAGIC data analysis. The current
  setup includes a
• 40 double 3.2 GHz processor computers, 50
  TByte storage system and 20 TB Disks.
• The Center will be integrated in the European
  Data-Grid network

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Towards FP7

• TA weaknesses of FP6
• satellites not yet launched
• only small part of HESS and MAGIC data goes to
  guest programs

lt-- no more PAMELA
launched June 2006 AGILE launch end of March
2007 GLAST launch November 2007
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GLAST DATA POLICY
After the initial on-orbit checkout,
verification, and calibrations, the first year
of science operations will be an all-sky survey.
all GBM data released LAT data on flaring
sources, transients, and sources of interest
will be released, with caveats (see following
slide) first-year LAT individual photon
candidate events initially used for detailed
instrument characterization, refinement of the
alignment, and key projects (source catalog,
diffuse background models, etc.) needed by the
community. Individual photon data released at
the end of year one. Subsequent photon data
released immediately after processing. burst
alerts and repoints for bright bursts
extraordinary ToOs supported workshops for
guest observers on science tools and mission
characteristics for proposal preparation
Observing plan in subsequent years driven by
guest observer proposal selections by peer
review - default is sky survey mode. Data
released through the science support center
(GSSC).
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• Multiwavelength observations are key to many
  science topics for GLAST.
• GLAST welcomes collaborative efforts from
  observers at all wavelengths
• For campaigners information and coordination,
  see http//glast.gsfc.nasa.gov/science/multi

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EGRET

• 271 sources

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GLAST

• red 0.1-0.4 GeV
• green 0.4-1.6 GeV
• blue gt1.6 GeV

gt 9000 sources are foreseen
First GLAST Symposium Feb. 2007
http//glast.gsfc.nasa.gov/science/symposium/2007
/
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AGILE Data Policy

• AGILE data will be available through a Guest
  Observers Program (GOP) that will be open to the
  international astrophysical community.
• GOP data will be allocated through the DATA
  Allocation Committee (ADAC) by means of yearly AO.

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AGILE Data Policy (2)

• Data rights for Targhet of Opportunity (TOO)
  sources belongs to the proposers thereof with
  participation of AGILE Team members who are
  essential for data processing.
• Some items belong to the AGILE Team
• Diffuse Radiation,
• Extragalactic background,
• Unidentified transient sources

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PAMELA Data Policy

• The PAMELA scientific primary goals are the
  search for heavy nuclei and non baryonic
  particles outside the Standard Model, for the
  understanding of the formation and evolution of
  our Galaxy and the Universe and for the exploring
  of the cycles of matter and energy in the
  Universe.
• Additional objectives of PAMELA are the study of
  galactic cosmic rays in the heliosphere, Solar
  flares, distribution and acceleration of solar
  cosmic rays (SCR's) in the internal heliosphere,
  magnetosphere and magnetic field of the Earth,
  stationary and disturbed fluxes of high energy
  particles in the Earth's magnetosphere and
  anomalous component of cosmic rays.
• Alerts for transient events, Solar flares will be
  immediately available on-line, or through other
  appropriate data distribution means within the
  limits of the resources available

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--gt only small part of HESS and MAGIC data goes
to guest programs

• Possible solution
• HESS, MAGIC, ARGO data not public but exchange
  between the experiments
• insertion in the data base of HESS MAGIC PAMELA
  and ARGO published data for cross-correlation
  with AGILE and GLAST data
• organize from now Data Policy for CTA

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http//www.roma2.infn.it/SciNeGHE07/
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Roma International Conference on Astroparticle
Physics Roma 20-22
June 2007

• http//www.ricap-conference.it